g140l-b grating calibration & qualification test results · g140l-c grating calibration &...

G140L-C Grating Calibration & Qualification Test Results

Date: December, 20, 2000Document Number: COS-03-0071Revision: Initial ReleaseContract No.: NAS5-98043CDRL No.: N/A

Prepared By:S. Osterman, COS Optical Scientist, CU/CASA Date

Reviewed By:K. McFeely, Optical Designer, BATC Date

Reviewed By:D. Ebbets, Calibration Scientist, BATC Date

Reviewed By:E. Wilkinson, COS Instrument Scientist, CU/CASA Date

Approved By:J. Andrews, COS Experiment Manager, CU/CASA Date

Approved By:J. C. Green, COS Principal Investigator, CU/CASA Date

Center for Astrophysics & Space AstronomyUniversity of Colorado

Campus Box 593Boulder, Colorado 80309

REVISIONSLetter ECO No. Description Check Approved Date

- Initial Release

Original Release THE UNIVERSITY OF COLORADOName Date At Boulder

Drawn: S. Osterman 12-20-00 The Center for Astrophysics and Space AstronomyReviewed: G140L-C Grating Calibration &Approved: Qualification Test Results

Size Code Indent No. Document No. Rev

A COS-03-0071 -Scale: N/A

COS-03-0071December 20, 2000

Center for Astrophysics & Space Astronomy Initial Release

G140L-C Grating Calibration &Qualification Test Results

University of Colorado at Boulder Page i

Table of Contents

1. G140L-C Characterization Overview ......................................................................... 12. CASA FUV/EUV Optics Test Facility ....................................................................... 33. G140L-C Imaging and Resolving Power Characterization......................................... 4

3.1 Test Setup................................................................................................................ 43.2 Search Pattern and Data Reduction......................................................................... 6

4. G140L-C Efficiency Measurement ........................................................................... 134.1 Test Setup.............................................................................................................. 134.2 Data Acquisition.................................................................................................... 144.3 Data Reduction...................................................................................................... 15

5. G140L-C Scatter Measurement................................................................................. 22

Table of Appendices

Appendix A: Witness Coupon Measurements .................................................................. 23Appendix B: NVR Witness Plate Results ......................................................................... 24Appendix C: List of Files Used in Resolution, Scattered Light and Efficiency Analyses 29

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University of Colorado at Boulder Page ii

Abbreviations and Acronyms

Å AngstromsARL CASA Astrophysical Research LaboratoryATP Assembly and Test ProcedureBASD Ball Aerospace Systems DivisionCASA Center for Astrophysics and Space AstronomyCOS Cosmic Origins SpectrographCU University of ColoradoDLD Delay Line DetectorFUSE Far Ultraviolet Spectroscopic ExplorerFWHM Full Width at Half MaximumHST Hubble Space TelescopeGROVER Grating Optical Verification Equipment/ReflectiveLASP Laboratory for Atmospheric and Space PhysicsMCP Microchannel PlateNVR Non-Volatile ResidueROI Region of Interest

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University of Colorado at Boulder Page 1

1. G140L-C CHARACTERIZATION OVERVIEW

G140L-C is the second of the G140L gratings to be characterized for the COSinstrument, and appears satisfactory in all respects. Tests performed include full gratingimage characterization, local efficiency measurements and full grating in-band scatter.The tests were performed at the CASA/ARL FUV/EUV optical test facility between 9March 2000 and 21 April 2000. The tests performed are listed in Table 1, and the resultsare summarized in Table 2 through Table4. All data files used in these analyses are listedin Appendix D.

Table 1: G140L Grating Tests Requirements

Test Optical Configuration Requirement Test PointsImagingandResolution

Modified Rowland Circle –Flight-like illuminationusing GROVER abberatedsource to simulate HSToptical system.

Demonstrate at least 2,000resolution across bandpass.If possible, data will be usedto select flight optic.

3 wavelengthsseparated byno less than100Å and nomore than250Å

First OrderGratingEfficiency

Wadsworth configuration. A10 mm beam illuminateslimited area of grating atseveral locations withgrating angle and detectorposition adjusted to simulateflight illumination angle ofincidence.

Demonstrate that gratingefficiency is abovespecification and determineefficiency in sufficientdetail to aid flight opticselection.

3×3 grid and 5wavelengthsseparated byno more than250Å,spanning atleast 600 Å ofthe passband.

Non-FirstOrderGratingEfficiency

Same setup as for FirstOrder Grating Efficiency

Measure grating response inas many orders as ispractical near 1400Å.

Test grating atonewavelengthand one point,at least in the0 and +2orders

GratingScatter

Analysis of data acquired inimaging and efficiencytests.

Demonstrate that gratingscatter is ≤2×10-5/Å 50Åaway from test line.

Analysis of atleast two testpoints or fullgrating

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Table 2: Grating Resolution Test Results

Wavelength FWHM(mÅ)

Resolutionλ/∆ λλ/∆ λλ/∆ λλ/∆ λ

1219.49Å 0.325Å 37501378.96Å 0.302Å 50501524.73Å 0.378Å 4040

Table 3: First Order Grating Efficiency Test Results

Wavelength(Å, Source)

First Order GratingEfficiency (Grating

Average)

MeasurementUncertainty

1048 (Ar) 0.047 --1164 (Kr) 0.256 0.8901236 (Kr) 0.314 1.2651304 (O) 0.326 1.1451470 (Xe) 0.312 1.1401565 (CO) 0.296 1.0211734 (CO) 0.269 1.0001935 (CO) 0.238 0.841

Table 4: Grating Scatter Test Results

SourceWavelength

(Å)

Source Counts(background

corrected)

ScatterWavelength

(Å)

Scatter Counts(background

corrected)Scatter/Å

1141.1-1191.1 37212 1140.1± 3.4 Å 2.9/6.8Å 1.1×10-5

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2. CASA FUV/EUV OPTICS TEST FACILITY

All testing of the flight optics must be performed in vacuum. The CASAFUV/EUV Optics Test Facility vacuum chamber is 11’ diameter by 14’ long, cryo-pumped and fitted with a 5’ by 10’ vibration isolated optics bench. The grating is eitherilluminated by the GROVER aberrated light source or by a monochromatic beam, and thelight is monitored by one of two open face microchannel plate detectors (figure 1).

VibrationallyIsolated OpticsBench

0.2m Monochromatorwith Flowing GasDischarge Source

3m Diameter Vacuum Chamber Opening into Class1000 Clean Room

Grating ImagingTest Beam Path

Grating Efficiency Beam Path

Witness coupons mountedin grating bezel holderupper coupon: CW-60 (monitor)lower coupon: CW-46 (integrator)

G140L-C Grating

NVR Witness Plate

Figure 1: Optics Test Facility

Cleanliness is monitored via two TQCMs, one mounted on the optics bench nextto, and with the same view factor as the test optic, and another over the bench lookingdown. Additional cleanliness monitoring is achieved by maintaining a non-volatileresidue (NVR) witness plate in the chamber and by keeping two witness mirrors in thechamber mounted with the grating. The NVR plates are rinsed before and after gratingtesting, and one of the witness mirrors is tested for reflectivity degradation at the end ofthe test cycle. The results of the NVR rinses and the reflectivity tests are included asappendices.

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3. G140L-C IMAGING AND RESOLVING POWERCHARACTERIZATION

3.1 TEST SETUP

The FUV gratings are designed to correct for the HST aberration. Consequently,it is necessary to illuminate the gratings with a similarly aberrated UV light source inorder to accurately assess the grating imaging and dispersion characteristics. This isaccomplished by using the Grating Optical Verification Equipment-Reflective(GROVER) optical subsystem developed by Kevin Redman, described in NSI document33-07-1101. GROVER is a finite conjugate system designed to simulate the spherically-aberrated, f/24 HST image at the input aperture of the COS-FUV subsystem. It was builtfrom the spare optics procured for the Reflective Aberration Simulator/Calibrator(RAS/CAL), which was used for testing the Space Telescope Imaging Spectrograph andthe Advanced Camera for Surveys instruments. GROVER uses the spare aspheric, conic,and turning mirrors in order to provide a chief ray to the grating under test whichprecisely matches the aberration content and input angle corresponding to the HST fieldpoint at the COS entrance aperture.

The aspheric mirror provides the appropriate spherical aberration into the image,while careful adjustment of the conic mirror position and tilt angles provide the correctcoma and astigmatism for the desired field point (the aperture stop is located immediatelyin front of the conic mirror). The turning mirrors were used to decrease the overall size ofthe system (in order to fit on the CU test table) and to provide the desired chief ray angle.The light source for GROVER is a sealed hollow cathode platinum lamp with amagnesium fluoride window. The test setup is shown in figures 2 and 3.

Vibrationallyisolated opticsbench

G140L on 4-Axismanipulator stage(three translationand one rotation)

Efficiency detector(not used for this measurement)

Delay line detector for imaging testson 2 axis translation stage

Grover opticalsubsystem

0.80 mmfield stop

Figure 2: Grating Imaging and Resolution Test Setup

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Delay Line Detector

0.8mm Field Stop

GROVER Optical Subsystem

10mm Aperture for Efficiency Beam Path

G130M-C Grating in mount

Figure 3: Photograph of G130M-C grating test setup installed in vacuum chamber.(G140L-C similar)

Light from the GROVER optical subsystem illuminates the test optic, which thendiffracts the light onto a Siegmund Scientific delay line detector with 25micron resolutionin the dispersion direction (the detector pixel size is approximately 2.4 microns, orapproximately 30-31mÅ/pixel). The GROVER system is placed so that it fullyilluminates the test optic with the GROVER prime focus the same distance from thegrating center as the HST focus would be on orbit. The test optic is rotated to thenominal angle α and the detector is located so as to be tangent to the focal surface at thenominal β value and at the required distance from the test optic. The location of the testoptic and the detector relative to the GROVER focus and optical path are initiallydetermined using theodolite metrology and knowledge of the GROVER system acquiredprior to delivery, and are as close to the flight geometry as possible. Fine adjustment ofthe focus is accomplished by translating the grating and detector during vacuum testing.The focal plane of the detector is not curved to match the focal surface of the grating.Consequently, once the best focus is determined at one wavelength, the detector must betranslated both tangent to and along the beam path in order to optimize the image for any

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other wavelength without any further adjustment of the grating position with respect tothe incident beam.

The test detector has a potassium bromide photcathode. Consequently, itsquantum efficiency falls off rapidly above 1550Å and so it is not possible to performimaging tests using the GROVER optical system and this detector at longer wavelengths.Therefore, no lines beyond 1525Å were analyzed for optimum resolution.

3.2 SEARCH PATTERN AND DATA REDUCTION

Images were recorded for 100 seconds (this allowed 10,000 counts in the selectedanalysis lines) and saved in FITS format. These were then read into IDL and the line ofinterest was selected manually (figure 4). The software then extracted the data within a250 pixel wide by 30 pixel high box centered on the selected feature. This subset wascollapsed along the dispersion axis and the resulting histogram was fit to a Gaussianprofile. This is repeated over a grid in grating translation (both across and parallel to thedispersion axis, as well as in grating piston) and detector translation

Once a reasonable line profile is obtained (compare figures 5-7, obtained nearfocus, with figure 8 obtained far from focus), the line width versus position can beanalyzed and the best profile for a given scan selected. This process is repeated in all thescan directions mentioned above until a minimum is located.

Line width is determined by fitting a Gaussian profile to the simple histogramcollapse of the image (no curvature correction or line rotation was used):

I(p)=I0exp(-((p-p0)/σ)2/2)

I(p) is the intensity at pixel p, p0 is the fit line center, I0 is the line maximum and σ is theGaussian width (I(σ)=I0e-½). The reported full width at half of the maximum (FWHM) iscalculated to be 2.354 times the Gaussian width σ. The full spectra are analyzed todetermine the local dispersion relation from known platinum lines at best focus and this isused to calculate the line width ∆λ from the FWHM in pixels. Finally grating resolvingpower can be calculated as R=λ/∆λ. This line width represents the product of the gratingresolving power, the detector resolution, and the finite extent of the GROVER source.No effort was made to extract the line broadening contribution due to detector resolution,since it is not well characterized, but is comparable to the flight detector resolution. TheGROVER source size contribution, on the other hand, is well know, and shouldcorrespond to a 0.029 arc second top hat, which in turn corresponds to a 3.3 pixel FWHMon the test detector. The resolutions quoted below represent the resolution without

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correcting for the detector broadening or source size in bold, and the resolution calculatedby subtracting the source width in quadrature below in parentheses.

Table 5a: Detailed resolution results showing best resolution achieved.

Image ID(yyyymmdd_

hhmmss_…)

LineCenter(pixel)

Wavelength(Å)

GaussianLine

Width(pixels)

FWHM(pixels)

LocalDispersion(Å/pixel)

FWHM(Å)

Resolution(λ/∆λλ/∆λλ/∆λλ/∆λ)

20001020_095348_dld.fit

(fig. 5)8551.1 1219.49 4.558 10.73 0.0303 0.325 3750

(3940)

20001020_095003_dld.fit

(fig. 6)13786.4 1378.96 4.198 9.88 0.0305 0.302 5050

(5350)

20001020_093409_dld.fit

(fig. 7)18522.8 1524.73 5.247 12.35 0.0306 0.378 4040

(4190)

(The value shown for the resolution in bold represents the resolutioncalculated using the full line width as observed, and the larger valueshown in parentheses below is the estimated resolution after removing thecontribution to the line width from the finite size of the GROVER source.)

The image heights are quite similar to those predicted by ray trace (approximately330, 200 and 90µm at 1219, 1379 and 1525Å, respectively, compared with the expected340, 180 and 30µm). (This assumes that the cross dispersion asymmetry is attributable tothe observed top to bottom asymmetry the source.)

Resolution as a function of grating cross dispersion motion was examined tovalidate the planned detector lifetime image motions. The results of this will besummarized in a separate report.

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Figure 4: Spectra recorded near the best foci for the grating position taken to be optimalwith the lines selected for analysis indicated. Typically, the brightest line in a givenspectrum was not the best line for analysis, either because it was inherently broad (as inthe case of the N-I triplet at 1200Å) or because it was part of an unresolved or poorlyresolved multiplet (Pt-I 1289.95/1290.01, for example). Platinum wavelengths are takenfrom Reader, et al., 1990.

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Figure 5: Pt-I 1219.50Å at best focus achieved. FWHM=0.325Å (3750 resolution)

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Figure 8: Pt-I 1378.96Å out of focus showing grossly asymmetric line profile (thisimage is from G140L-B; G140L-C out of focus images are similar).

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4. G140L-C EFFICIENCY MEASUREMENT

4.1 TEST SETUP

The purpose of these tests was to determine the grating efficiency of the G140Loptic by measuring the efficiency of a small portion of the optic at nine points spanningthe blazed surface and forming a 3×3 grid. Measurements were performed at sixwavelengths within the nominal bandpass separated by no more than 250Å. The gratingwas illuminated by a quasi-parallel, 10mm diameter, monochromatic beam at the desiredtest wavelength and at the nominal incident angle (α =7.408º). The light source was aflowing gas discharge lamp (the gases used for each test wavelength are listed in table 3).

The test detector (Quantar model 3391 MCP imaging detector) was placed on aURM-100 rotation stage which in turn rode on top of a GV-88 translation stage. Thetranslation and rotation stage allowed the detector to be either positioned between the testoptic and the light source viewing the direct beam or close to the Wadsworth focus forthe test grating. The GV-88 translation rail was installed roughly tangent to theWadsworth focal surface at the central wavelength. Care was taken to ensure that thesame portion of the detector was illuminated in both configurations and at the same angleof incidence. However, since the grating serves to focus the incident beam, a detectorsensitivity map was applied to the data to correct for spatial variations in the detectorresponse. Grating tilt was manually adjusted between vertical rows of the 3×3 grid inorder to ensure that the detector was properly illuminated. Finally, care was taken toensure that the detector is illuminated at the same angle of incidence for allmeasurements, both by analysis of the expected light path, and by direct observation ofthe detector response versus angle in the incident and diffracted viewing modes. The testsetup is illustrated in figure 9.

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Collimated light from 0.2m monochromator

2-10 mm apertures

Quantar detector positioned to view diffracted light

Quantar detector positioned to viewdirect illumination

Efficiency Beam Path - Direct Beam Sampling

Efficiency Beam Path - Diffracted Beam Sampling

Transfer mirrors

Figure 9: Grating efficiency test setup. Light from a monochromator is directed into thetest chamber so as to illuminate a small portion of the grating in a Wadsworthconfiguration. In addition to being able to measure the first inside order efficiency(m=+1), this setup can observe m=0,-1,± 2 and –3 orders due to the low incident angleand low dispersion of the G140L gratings.

4.2 DATA ACQUISITION

Data was acquired in three distinct operations, one for each vertical row of thedetector. Between rows, the vacuum chamber was backfilled and the grating tilt (rotationabout the horizontal tangent to the grating) was manually corrected. Within each row, theefficiency of the three points was measured one wavelength at a time as follows: oncethe lamp had been given time to stabilize and the line had been peaked up on themonochromator, a background (dark) image was recorded. Next the incident beam wasobserved and an image recorded. The detector was translated and rotated to observe thediffracted beam from the first horizontal position and another image was recorded. The

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detector was then returned to the original position and another direct beam image wasrecorded. Next, the grating was translated to illuminate the next spot and the diffractedbeam observed and recorded, and another incident beam was recorded. Finally, thegrating was moved to the final location, the diffracted beam recorded and the incidentbeam recorded. Before moving on to the next wavelength a final background wasrecorded.

By recording an incident beam image immediately before and after eachdiffracted beam image, it was possible to correct for slow drift in the lamp output. Thebackground images were used to correct for detector dark counts and to monitor detectorhealth. Additional images were taken when there was concern that light from otheremission lines might be contaminating the incident beam.

Prior to data acquisition, spectra were recorded with the test detector for all thegasses (emission line sources) to be used in the efficiency measurements. These spectrawere used to select the brightest, most isolated emission features for use in the analysis.In all cases the background between lines fell to detector background levels.

4.3 DATA REDUCTION

Each data point (both spatial and in wavelength) had associated with it at least 4images: one or two background images, an initial and a final incident beam image and adiffracted beam image. The ‘spot’ of light in each image was identified, marked and thecounts in that region were totaled (as well as corrected for interface deadtime (0.3-0.7%)and spatial detector response variation (± 5%RMS)). The counts outside the region ofinterest (ROI) were also totaled. Next, the background for each image was determined byapplying the ROI’s for the incident and diffracted beams to the background images. Theratio of the ROI to non-ROI count rates was determined for the background images, andthis ratio multiplied by the non-ROI count rates in each illuminated image to estimate thebackground contribution to the image in the ROI. This background count rate could thenbe subtracted from the ROI count rate to yield the incident and diffracted count rates.With this information, the local efficiency was calculated as follows:

ε(i,j,λ) = D(i,j,λ)/((I0(i,j,λ)+ I1(i,j,λ))/2)

Where ε(i,j,λ) is the calculated efficiency at position i,j, wavelength λ. D(i,j,λ) isthe background corrected diffracted beam count rate and I0(i,j,λ) and I1(i,j,λ) are theinitial and final background corrected incident beam count rates. A typical image set isshown in figure 10.

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Images were integrated for 100 to 500 seconds, depending on count rate, so that atleast 10,000 counts were recorded in each diffracted image, and all images for a givendata set were recorded for the same time period. Drift in the lamp was typically less than1% between incident images (except as noted below). Statistical uncertainties wereanalyzed in accordance with Bevington (1969). An additional 1% uncertainty was addedin quadrature to represent uncertainty in the flat field correction. The uncertainty in thelamp output was modeled as half the variation in the initial and final incident count ratesand this was also added to the uncertainty in quadrature. No uncertainty was included forthe linearity correction, since this would be of order .01%. Finally, a 3% uncertainty wasadded to represent a disagreement between CASA and GSFC witness coupon reflectivitymeasurements. In most cases this is the dominant source of uncertainty.

Table 6: G140L-C Grating Efficiency.

Wave-length

(Å)

MinimumReq.

Efficiency

CoatingReflectivity

GratingBlaze

Efficiency

PredictedEfficiency

ObservedEfficiency

Statisticaluncertainty(absolute)

EfficiencyRMS

variation1048 (NA) (NA) (NA) (NA) 0.047 0.002 (NA)1164 (NA) 0.747 0.371 0.277 0.256 0.890 1.6921236 0.246 0.858 0.371 0.318 0.314 1.265 2.3061304 0.245 0.856 0.370 0.317 0.326 1.145 2.0991470 0.244 0.853 0.369 0.315 0.312 1.140 1.4551565 0.244 0.851 0.369 0.314 0.296 1.021 1.3481734 0.243 0.849 0.338 0.287 0.269 1.000 1.2761935 0.241 0.849 0.293 0.249 0.238 0.841 0.743

Values cited are absolute efficiency. Uncertainties and variations cited areabsolute rather than relative. The minimum required efficiencies are based on predicteddetector performance and telescope throughput. The coating reflectivity and grating blazeefficiency values cited are interpolated from Goddard and J-Y test data. The predictedefficiency is the product of the coating reflectivity and the blaze efficiency. Theobserved efficiency is the average of all data points excluding the center (which will notbe illuminated in flight. The statistical uncertainty is the average of the individualuncertainties as described in the text and the efficiency variation is the RMS variationacross the grating. Efficiency at 1048 was measured at only one point on the grating.

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Table 7: G140L-C Grating Efficiency at 1470Å for various spectroscopic ordersmeasured at a single point (grating top center).

SpectroscopicOrder

ObservedEfficiency at 1470Å

1 0.324-1 0.3120 0.048-3 0.0292 0.003-2 0.005

Figure 10: Images taken for the 1304Å, grating center efficiency measurement set. Thecount rates in the figures are flat field corrected (note that only one of two backgroundimages is shown here). The linearity and background corrections are not indicated.Actual images are circular (the apparent distortion is due to plot aspect ratio).

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Figure 11: Mean efficiency of the grating at the test wavelengths compared to theexpected efficiency and required efficiency. Measured efficiency is the average of allmeasurements excluding the center (which will not be illuminated in flight).

Note the drop in reflectivity from the top to the bottom of the grating at all wavelengths(figures 12-18). This is unique to this optic in appearing at all wavelengths and with suchlarge variation.

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Figure 12: Efficiencies measured at each point on the grating. Illustration in lower leftcorner of the plot shows the location where each data set was taken, as well asapproximate beam size. The darker line marked with squares is the grating average.

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University

Figure 13: Measured efficiencies(uncertainties) at 1164Å.


of Colorado at Boulder




Page 20

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Universit

Figure 17: Measured efficiencies
(uncertainties) at 1565Å.



y of Colorado at Boulder Page 21

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5. G140L-C SCATTER MEASUREMENT

Prior to realigning the grating for the second efficiency data row, several deepimages were taken with the imaging setup (see figure 2). Twenty two 100-200 secondintegrations were recorded near the optimum focus. These photon lists were thenconcatenated after correcting for image motion and used to produce a single deepexposure. This region was selected because the platinum lamp window and condenserwhich feed the GROVER subsystem are made of MgF2, and so no light below 1145Åshould be transmitted to the diffraction grating. As a result, it is reasonable to assumethat any counts recorded below 1145Å on the detector must be either detectorbackground or scattered light. By comparing the counts in this region with all the countsoccurring within ±50Å (only +50Å need be considered) and a representativeunilluninated portion of the detector, we can estimate the grating scatter to beapproximately 9 ×10-6/Å within ±50Å. The analysis is illustrated in figure 20 and in table4 (p. 2).

Figure 20: G140L-C Grating Scatter.

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Appendix A: Witness Coupon Measurements

Witness coupons CW-46 and CW-60 followed G140L-C bonding and testing. Theremaining coupons remained in dry storage except for periodic testing. There appears tohave been a substantial drop in reflectivity at shorter wavelengths in all samples. This isdifficult to explain, as there were no anomalies in the vacuum system operations andQCM and NVR results were nominal. Also, the drop in reflectivity appears in allsamples (not just those used in the grating bonding and testing), and after both bondingand testing.

Percent Reflectivity / Change in ReflectivityID Date1216Å 1435Å 1608Å 1750Å 1950Å 1991Å 2046Å 2537Å 3131Å

Function

8/24/2000 (prebond)

83.99 86.50 84.01 82.46 81.76 82.45 83.58 87.80 89.53

9/05/2000 (postbond)

83.59 86.08 83.39 82.77 81.31 81.94 83.23 87.46 88.76

11/28/2000 (posttest)

83.02 85.21 82.24 82.42 81.34 81.86 82.96 87.46 89.11

CW-41

Change inreflectivity

-0.97 -1.29 -1.77 -0.03 -0.42 -0.59 -0.62 -0.34 -0.43

G140L-Ccoupon

Remained inshippingcontainer

8/24/2000 (prebond)

85.09 86.46 83.74 82.35 82.098 82.70 83.90 88.41 90.07


84.81 85.86 83.48 82.52 81.845 80.97 83.94 88.14 89.77

11/28/2000 (posttest)

83.65 84.19 81.53 82.01 81.75 82.26 83.38 87.89 89.68

CW-63


-1.44 -2.27 -2.21 -0.35 -0.35 -0.44 -0.52 -0.52 -0.38

G140L-Ccoupon


8/24/2000 (prebond)

84.22 85.69 83.20 82.00 79.83 80.57 82.29 88.00 89.77


83.67 83.93 82.70 82.01 81.15 80.26 83.38 87.56 89.75

11/28/2000 (posttest)

82.79 83.07 80.67 81.10 80.80 81.20 82.23 86.89 88.84

CW-79


-1.43 -2.62 -2.54 -0.90 0.97 0.62 -0.06 -1.11 -0.93

G140L-Ccoupon


8/24/2000 (prebond)

83.03 85.92 84.18 82.76 79.96 80.57 82.23 87.92 89.65


84.08 85.96 83.23 82.24 81.91 80.27 83.76 87.56 89.38

11/16/2000 (posttest)

82.74 83.57 81.08 81.51 80.64 80.84 81.96 87.07 89.13

CW-46


-0.29 -2.35 -3.09 -1.25 0.68 0.27 -0.27 -0.84 -0.52

G140L-Ccoupon

Followedbonding

and opticaltesting

8/24/2000 (prebond)

84.83 87.18 84.58 83.03 82.19 82.38 83.98 87.95 89.56


84.08 86.37 83.17 82.87 81.62 82.31 83.50 87.60 89.52

11/16/2000 (posttest)

83.70 84.92 81.65 81.98 81.11 81.22 82.33 87.41 89.02

CW-60


-1.13 -2.26 -2.93 -1.05 -1.08 -1.16 -1.65 -0.54 -0.54

G140L-Ccoupon

Followedbonding

and opticaltesting

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Appendix B: NVR Witness Plate ResultsA 12” square stainless steel witness plate was installed in the vacuum chamber beforetesting on the G140L-C grating was begun (at the conclusion of G140L-C testing), andthen rinsed at the conclusion of testing. Rinses were performed on 27 September, 2000(pretest) and on 2 November, 2000 (post test).

Results of the NVR rinses appear on the following pages.

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Appendix C: List of Files Used in Resolution, Scattered Light and EfficiencyAnalyses

G140L-C Resolution Analysis FilesNote: No flatfield used in analysis

Wavelength File Name1219.5Å 20001020_095348_dld.fit1378.96Å 20001020_095003_dld.fit1509.29Å 20001020_093409_dld.fit

G140L-C Scattered Light Analysis FilesNote: No flatfield used in analysisAll images taken within 2mm of focus. Images offset and concatenatedto form large metafile prior to scattered light analysis.

20001020_085347_dld.fit 20001020_092637_dld.fit 20001020_095728_dld.fit20001020_085810_dld.fit 20001020_093022_dld.fit 20001020_100115_dld.fit20001020_090154_dld.fit 20001020_093409_dld.fit 20001020_100459_dld.fit20001020_090626_dld.fit 20001020_093758_dld.fit 20001020_100837_dld.fit20001020_091009_dld.fit 20001020_094153_dld.fit 20001020_101257_dld.fit20001020_091454_dld.fit 20001020_094603_dld.fit 20001020_170502_dld.fit20001020_091847_dld.fit 20001020_095003_dld.fit20001020_092240_dld.fit 20001020_095348_dld.fit

COS-03-0071December 20, 2000




G140L-C Efficiency analysis filesFlatfield used in analysis: flatfield_20000616_30deg.fitNote: Total counts is the raw total image counts includingcounts outside of the actual illuminated area.

Wavelength: 1048 Emission source: ArgonImage Location: Gx:0.000000 Gy: 0.000000

Image Type File Name TotalCounts

Background 20001023_161755_rae.fit 1846Background 20001023_170532_rae.fit 1924

Incident 20001023_162920_rae.fit 12857Incident 20001023_165450_rae.fit 13211

Diffracted 20001023_164311_rae.fit 3158

Wavelength: 1164 Emission source: KryptonImage Location: Gx:0.000000 Gy: 0.000000





Wavelength: 1164 Emission source: KryptonImage Location: Gx:-23.0000 Gy: 0.000000





COS-03-0071December 20, 2000









Wavelength: 1164 Emission source: KryptonImage Location: Gx:0.000000 Gy: -18.0000





Wavelength: 1164 Emission source: KryptonImage Location: Gx:-18.0000 Gy: -18.0000










COS-03-0071December 20, 2000




Waelength: 1164 Emission source: KryptonImage Location: Gx:0.000000 Gy: 20.0000















COS-03-0071December 20, 2000
























COS-03-0071December 20, 2000




Wavelength: 1264 Emission source: KryptonImage Location: Gx:-18.0000 Gy: -18.0000















COS-03-0071December 20, 2000














Wavelength: 1304 Emission source: OxygenImage Location: Gx:0.000000 Gy: 0.000000





Wavelength: 1304 Emission source: OxygenImage Location: Gx:-23.0000 Gy: 0.000000





COS-03-0071December 20, 2000









Wavelength: 1304 Emission source: OxygenImage Location: Gx:0.000000 Gy: -18.0000





Wavelength: 1304 Emission source: OxygenImage Location: Gx:-18.0000 Gy: -18.0000





COS-03-0071December 20, 2000




Wavelength: 1304 Emission source: OxygenImage Location: Gx:18.0000 Gy: -18.0000










Wavelength: 1304 Emission source: OxygenImage Location: Gx:-18.0000 Gy: 20.0000










COS-03-0071December 20, 2000




Wavelength: 1470 Emission source: XenonImage Location: Gx:0.000000 Gy: 0.000000





Wavelength: 1470 Emission source: XenonImage Location: Gx:-23.0000 Gy: 0.000000










Wavelength: 1470 Emission source: XenonImage Location: Gx:0.000000 Gy: -18.0000





COS-03-0071December 20, 2000




Wavelength: 1470 Emission source: XenonImage Location: Gx:-18.0000 Gy: -18.0000





Wavelength: 1470 Emission source: XenonImage Location: Gx:18.0000 Gy: -18.0000










Wavelength: 1470 Emission source: XenonImage Location: Gx:-18.0000 Gy: 20.0000





COS-03-0071December 20, 2000









Wavelength: 1565 Emission source: Carbon MonoxideImage Location: Gx:0.000000 Gy: 0.000000





Wavelength: 1565 Emission source: Carbon MonoxideImage Location: Gx:-23.0000 Gy: 0.000000










COS-03-0071December 20, 2000




Wavelength: 1565 Emission source: Carbon MonoxideImage Location: Gx:0.000000 Gy: -18.0000





Wavelength: 1565 Emission source: Carbon MonoxideImage Location: Gx:-18.0000 Gy: -18.0000















COS-03-0071December 20, 2000
























COS-03-0071December 20, 2000




Wavelength: 1470 Emission source: XenonImage Location: Gx:0.000000 Gy: 18.0000+1 Order





Wavelength: 1470 Emission source: XenonImage Location: Gx:0.000000 Gy: 18.0000-1 Order





Wavelength: 1470 Emission source: XenonImage Location: Gx:0.000000 Gy: 18.00000 Order





COS-03-0071December 20, 2000









Wavelength: 1470 Emission source: XenonImage Location: Gx:0.000000 Gy: 18.0000+2 Order










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